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New Neighbours: IV. 30 DENIS Late-M Dwarfs Between 15 and 30 Parsecs

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New Neighbours: IV. 30 DENIS Late-M Dwarfs Between 15 and 30 Parsecs Astronomy & Astrophysics manuscript no. (will be inserted by hand later) New neighbours: IV. 30 DENIS late-M dwarfs between 15 and 30 parsecs N. Phan-Bao1,2, J. Guibert1,2, F. Crifo2, X. Delfosse3, T. Forveille3,4, J. Borsenberger5, N. Epchtein6, P. Fouqu´e7,8, and G. Simon2 1 Centre d’Analyse des Images, DASGAL, Observatoire de Paris, 61 avenue de l’Observatoire, 75014 Paris, France 2 Observatoire de Paris (DASGAL/UMR-8633), 75014 Paris, France 3 Laboratoire d’Astrophysique de Grenoble, Universit´eJ. Fourier, B.P. 53, F-38041 Grenoble, France 4 Canada-France-Hawaii Telescope Corporation, 65-1238 Mamalahoa Highway, Kamuela, HI 96743 USA 5 Institut d’Astrophysique de Paris, 98bis boulevard Arago, 75014 Paris 6 Observatoire de Nice, BP 4229, 06304 Nice Cedex 4, France 7 DESPA, Observatoire de Paris, 5 place J. Janssen, 92195 Meudon Cedex, France 8 European Southern Observatory, Casilla 19001, Santiago 19, Chile Received / Accepted Abstract. We present 30 new nearby (d < 30 pc) red dwarf candidates, with estimated spectral types M6 to M8. 26 were directly selected from the DENIS database, and another 4 were first extracted from the LHS catalogue and cross-identified with a DENIS counterpart. Their proper motions were measured on the MAMA measuring ′′ − machine from plates spanning 13 to 48 years, and are larger than 0.1 yr 1, ruling out the possibility that they are giants. Their distances were estimated from the DENIS colours and IR colour-magnitude relations and range between 15 and 30 pc. Key words. astrometry - proper motions - low mass stars 1. Introduction For the most part the known members of the so- lar neighbourhood have been selected within the avail- Much of our understanding of stellar astronomy rests able catalogues of trigonometric parallaxes, though some arXiv:astro-ph/0110583v1 27 Oct 2001 upon the nearest stars. As individual objects they are the significant fraction is still included on the basis of pho- brightest and hence best studied examples of their spec- tometric or spectroscopic distances (Gliese 1956; Gliese tral type, and their trigonometric parallaxes can be mea- & Jahreiß 1979, 1991). However, for at least the last sured accurately, although with significant effort. The so- fifty years, parallax programs have selected their targets lar neighbourhood sample also provides deep insight into for a good part from proper motion catalogues, such as the nature of our Galaxy’s components, through studies of the Cincinnati catalogues (Porter et al. 1918, 1930), the its stellar luminosity and mass functions, its kinematics, Luyten catalogues (LFT 1955; LTT 1957, 1961; LHS 1979; chemical composition, and multiplicity statistics. NLTT 1980) or the Lowell catalogues (Giclas et al. 1971, Perhaps surprisingly, this sample is still incomplete, 1978). This leads to a proper motion bias of the resulting even very close to the Sun, as illustrated by the recent sample, at least for the faint end. To date even the smaller discoveries of three new stars with d < 6 pc (Henry et al. LHS catalogue has been incompletely followed-up, and the 1997; Delfosse et al. 2001; Scholz et al. 2001 ). ¿From a Luyten catalogues therefore contain many unrecognized comparison of the observed star densities within 5 and nearby stars (e.g. Scholz et al. 2001, for an extreme exam- 10 parsecs, Henry et al. (1997) estimate that approx- ple). Several groups are working to identify them (Henry imately 130 systems are missing from the 10 pc sam- et al. 1997; Gizis & Reid 1997; Jahreiß et al. 2001). One ple. Most of these missing stars are red M dwarfs, with limitation to these efforts is the much brighter limiting B−V > 1.70 (Gliese et al. 1986), and the deficit is largest magnitude of the proper motion catalogues south of dec- ◦ south of declination −30◦. lination −33 (e.g. Scholz et al. 2001, for a recent discus- sion), where a much larger fraction of the solar neighbour- hood stars is currently missing. Send offprint requests to: N. Phan-Bao, e-mail: [email protected] 2 N.Phan-Bao et al.: New neighbours: IV. 30 DENIS late-M dwarfs I−J Spectral type MI Dlim 2.0 M5.5 - M6 11.5 250 pc 2.5 M6.5 - M7 12.9 130 pc 3.0 M8 14.0 80 pc Table 1. Typical detection limiting distances (Dlim) for M dwarfs with colour 2.0 ≤ I−J ≤ 3.0 in the DENIS sur- vey. The spectral types are from Leggett (1992) and the absolute magnitude is taken from Figure 1. The recent near-infrared sky surveys, DENIS and 2MASS, represent a powerful alternative tool to identify these faint and cool nearby stars. Candidates are first se- lected on simple colour and photometric distance crite- ria, producing an initial list that also contains many gi- ants, and potentially some pre-main-sequence stars. At Fig. 1. MI : I − J HR diagram for M dwarfs with known low galactic latitudes it would also include many red- distances (from Leggett 1992 and Tinney et al. 1995). Our dened distant stars. In a second step these contaminat- empirical polynomial fit and the 3 Gyr model of Baraffe ing populations need to be rejected, through either (1) et al. (1998) for a solar metalicity are overlaid. a systematic spectroscopic follow up (Gizis et al. 2000), or (2) proper motion selection (distant giants have very small proper motions), or (3) more accurate multi-colour (J and Ks) and one optical band (I). DENIS observa- photometry than available from the surveys. Systematic tions are carried out on the ESO 1m telescope at La Silla. Dichroic beam splitters separate the three channels, and spectroscopy is clearly the cleanest approach, and does not ′′ reject the few nearby star that, like Gl 710 for instance, a focal reducing optics provide scales of 3 per pixel on the 256×256 NICMOS3 arrays used for the two infrared have small proper motions. Proper motion selection on ′′ the other hand is cheap and effective, but it obviously channels, and 1 per pixel on the 1024×1024 Tektronix does nothing to correct for the proper motion bias of the CCD detector of the I channel. present nearby star catalogues. The image data were processed with the stan- We are using here the DENIS near infrared sky survey dard DENIS software pipeline (Borsenberger 1997, to identify possible very-low-mass stars within 30 parsecs. Borsenberger et al., in preparation) at the Paris Data We conservatively adopt a distance cutoff slightly larger Analysis Center (PDAC). The thermal background pro- than the 25 pc limit of the Catalogue of Nearby Stars duced by the instrument and the sky emission is de- of Gliese and Jahreiß (CNS3, 1991), to avoid losing bona- rived from a local clipped mean along the strip. Flat- fide d < 25 pc stars from imprecise photometric distances. field corrections are derived from observation of the sun- One initial result of this effort was the discovery of an M9 rise sky. Source extraction and photometry are performed dwarf at a spectroscopic distance of only 4 pc, DENIS- at PDAC, using a space-varying kernel algorithm (Alard P J104814.7-395606.1 (Delfosse et al. 2001). In this paper 2000). The astrometry of the individual DENIS frames is ′′ we present 26 nearby red dwarf candidates, selected with referenced to the USNO-A2.0 catalogue, whose ∼ 1 ac- I−J > 2.0 (M6 or later) in the DENIS database and with curacy therefore determines the absolute precision of the a proper motion larger than 0.1′′yr−1. 13 of these are new, DENIS positions. and another 13 were known as high-PM objects but had With a 100% completeness level at I∼18.0, J∼16.0 and not been characterized further. Four additional candidates Ks ∼13.0, the DENIS survey is sensitive to M dwarfs out were first selected from the southern part of the LHS cat- to large distances (Table 1), well beyond the 25 pc limit alogue and then identified with DENIS counterparts. of the CNS3 (1991). In this part of the HR diagram the Sect. 2 reviews the sample selection, and Sect. 3 I−J (or alternately I−K) colour index is an excellent spec- presents the photographic photometry and the proper mo- tral type and luminosity estimator (Leggett 1992). The tion measurements. We discuss the results in Sect. 4 and DENIS data therefore provide immediate identification of summarize in Sect. 5. M dwarf candidates from I−J > 1.0, and, under the as- sumption that they are indeed dwarfs, a good estimate of their distance through colour-magnitude relations. Color- 2. Sample selection magnitude relations have yet to be established for the na- 2.1. DENIS observations tive DENIS photometric system, and we therefore resort to a relation in the standard Cousins-CIT system to de- The DEep Near-Infrared Survey (DENIS) is a southern rive distances for red stars in the DENIS database. A pre- sky survey (Epchtein 1997), which will provide full cover- liminary comparison of the two photometric systems for age of the southern hemisphere in two near-infrared bands very late M dwarfs shows differences of ∼0.1 mag between N.Phan-Bao et al.: New neighbours: IV. 30 DENIS late-M dwarfs 3 Table 2. Position and observation information for the 30 new nearby star candidates DENISName Othername α2000 δ2000 DENIS Number of Time Epoch observations baseline [yr] DENIS-P J0004575−170937 ... 00 04 57.54 −17 09 37.0 1999.521 4 47.834 DENIS-P J0013466−045736 LHS 1042 00 13 46.60 −04 57 36.5 1999.846 4 45.173 DENIS-P J0019275−362015 ... 00 19 27.53 −36 20 15.7 1999.877 3 21.064 DENIS-P J0041353−562112 ..
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